Pulsars as the Source of the WMAP Haze

Abstract

The WMAP haze is an excess in the 22 to 93 GHz frequency bands of WMAP extending about 10 degrees from the galactic center. We show that synchrotron emission from electron-positron pairs injected into the interstellar medium by the galactic population of pulsars with energies in the 1 to 100 GeV range can explain the frequency spectrum of the WMAP haze and the drop in the average haze power with latitude. The same spectrum of high energy electron-positron pairs from pulsars, which gives rise to the haze, may also generate the observed excesses in AMS, HEAT and PAMELA. We discuss the spatial morphology of the pulsar synchrotron signal and its deviation from spherical symmetry, which may provide an avenue to determine the pulsar contribution to the haze.

18 pages, 4 figures. Corrected errors in fig 1-3 and added discussion of the detailed spatial morphology of the haze signal

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Cited by in corpus (12)

• Giant Gamma-ray Bubbles from Fermi-LAT: AGN Activity or Bipolar Galactic Wind?
• Implications of CoGeNT and DAMA for Light WIMP Dark Matter
• Galactic Signatures of Decaying Dark Matter
• Investigating the Uniformity of the Excess Gamma rays towards the Galactic Center Region
• The Morphology of the Galactic Dark Matter Synchrotron Emission with Self-Consistent Cosmic Ray Diffusion Models
• Systematic effects in the extraction of the 'WMAP haze'
• The Mass Function of Void Groups as a Probe of the Primordial non-Gaussianity
• The Electron Injection Spectrum Determined by Anomalous Excesses in Cosmic Ray, Gamma Ray, and Microwave Signals
• Dark Matter Studies Entrain Nuclear Physics
• Testing the Dark Matter Annihilation Model for the WMAP Haze
• Cosmic ray backgrounds for dark matter indirect detection
• Synchrotron Emission From Young And Nearby Pulsars